NASA - National Aeronautics and Space Administration

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AMAZONIS PLANITIA -- Photo No. AC87-0279-8
Scene covers the boundary scarp between the ancient crate red highlands and the northern plains. The sedimentary deposits north of the highlands in Amazonis Planitia may consist of pyroclastic rocks or paleo-polar deposits. Ancient river channels cut the cratered highlands. (North is 107. clockwise.) (Viking Orbiter
picnos 690A02, 06, 08.) Image processing by Alfred McEwen, U.S.
Geological Survey, Flagstaff, Az.

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Photo No. AC85-0760-4 -- Early morning clouds in Noctis Labyrinthus on the Planet Mars.Condensate clouds are seen here in early morning in the canyons of Labyrinthus Noctis, which lies at the western end of the equatorial Valles Marineris system. This picture, which covers
about 90,000 km2, was made by combining three frames of the same field taken through violet, green, and red filters.

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MARINER 9, ORBIT 112 -- At right is a 80 x 40 mi. dune field of loose material in the floor of a 93 mile wide crater in the Hellespontus region of Mars, photographed by the Mariner 9 spacecraft's narrow an- gle camera. The dune field appears as a black spot, at left,
in a wide-angle photograph of the crater (arrow). The field is composed of numerous long dunes spaced about a mile apart. The lee slopes of the dunes appear brighter in this picture.

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Photo No. AC85-0760-2 -- Left: Photo of Martian crater above 30 degrees latitude shows softening of features, “creep deformation,” caused by ground ice.
Right: Martian crater below 30 degrees latitude shows no such softening.

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Photo No. AC87-0279-9 -- North polar ice cap of Mars as seen during mid summer in the northern hemisphere (Ls=118°).The reddish areas consist of eolian dust, bright white areas consist of a mixture of water ice and dust, and the dark blue areas consist of sand dunes forming a huge "collar" around the polar ice cap. (The colors have been
enhanced with a decorrelation stretch to better show the color variability.) Shown here is an oblique view of the polar region, as seen with the Viking 1 spacecraft orbiting Mars over latitude 39. north. The spiral bands consist of valleys which form by a combination of the Coriolis forces, wind erosion, and differential
sublimation and condensation.

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Photo No. AC76-1011-2-12 -- Typical Martian terrain near the Viking Lander 2 site shows rocks with vesicles, or small holes, in them. Such rocks on Earth can be produced by either high volcanic processes or by hypervelocity impacts of meteorites. Some areas are lighter than others, suggesting the presence of two kinds of fine-grained materials, which also can be produced by both. volcanic and impact processes.

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Photo No. AC87-0279-3 -- Mars Volcano
Olympus Mons is the largest volcano on Mars, possibly the largest in the Solar System. It is more than 372.84 miles (600 km) across and towers 16.8 mils (27 km) above the Mars surface level.

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Photo No. AC87-0279-7 -- Scene covers the boundary scarp between the ancient cratered highlands and the northern plains of Mars over an area east of Mangala Valles (latitude -7° to -3°, longitude 146° to 149°) . Ancient river channels run north through the ancient cratered highlands, but are covered north of the scarp by young lava flows. The large impact crater just north of the scarp shows flow-like ejecta lobes, which may form due to the presence of subsurface water or ice. (Viking Orbiter picnos 455S09-17, 456S13-20, 457S16-20.) Image processing by Alfred McEwen, U.S. Geological Survey, Flagstaff, Arizona.

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Photo No. AC87-0279-11 -- The large circular area with a bright yellow color (in this rendition) is known as Arabia. The boundary between the ancient, heavily-cratered southern highlands and the younger northern plains occurs far to the north (latitude 40.) on this side of the planet, just north of Arabia. The dark streaks with bright margins emanating from craters in the Oxia Palus region (to the left of Arabia) are caused by erosion and/or deposition by the wind. The dark blue area on the far right, called Syrtis Major Planum, is a low-relief volcanic shield of probable basaltic composition. Bright white areas to the south, including the Hellas impact basin at lower right, are covered by carbon dioxide frost.
This digital mosaic was produced by Jody Swann, using the PICS (Planetary Image Cartography System) image processing system developed at the U.S. Geological Survey in Flagstaff, Arizona

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Photo No. AC87-0279-2 -- Canyon floor of the Valles Marineris on Mars. Geologists believe the lakebed sediments have been deposited over the original canyon wall.

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Photo No. A85-0760-3 -- MARS
Martian Valley network channels (riverbeds).

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Photo No. AC87-0279-1 -- MARS WITH VALLES MARINARES
Scene covers show much of Mars including the Valles Marinares, a long, thin like feature in the center of the image. Image processing by the U.S.
Geological Survey, Flagstaff, Arizona.